I. Constellations
... ____stars____ named after ____an animal____, ____a person____ or ___ an object ____. B. In modern astronomy, a constellation is defined as a specific ____area____ of the sky as determined by the International Astronomical Union (IAU). C. The celestial sphere is divided into __88___ contiguous region ...
... ____stars____ named after ____an animal____, ____a person____ or ___ an object ____. B. In modern astronomy, a constellation is defined as a specific ____area____ of the sky as determined by the International Astronomical Union (IAU). C. The celestial sphere is divided into __88___ contiguous region ...
Distance determination for RAVE stars using stellar models
... The future prospects for distance determinations are very promising. In the next decade the Gaia satellite (Perryman et al. 2001) will observe up to 109 stars with exquisite astrometric precision. The mission is due to start in 2012, but a final data release will not arrive until near the end of the ...
... The future prospects for distance determinations are very promising. In the next decade the Gaia satellite (Perryman et al. 2001) will observe up to 109 stars with exquisite astrometric precision. The mission is due to start in 2012, but a final data release will not arrive until near the end of the ...
here
... minutes to 24.8 arc minutes but increases in illumination from 27% to 48% during the course of the month. As the sun rises in late May, Venus will reach an altitude of about 23 degrees for observers at 40 degrees north. The brightest planet is at the descending node on May 9th. On May 22nd, Venus li ...
... minutes to 24.8 arc minutes but increases in illumination from 27% to 48% during the course of the month. As the sun rises in late May, Venus will reach an altitude of about 23 degrees for observers at 40 degrees north. The brightest planet is at the descending node on May 9th. On May 22nd, Venus li ...
DUSTY CIRCUMSTELLAR DISKS B. Zuckerman
... It has not been easy to find old T Tauri stars, in the 10- to 20-million-year range, because such stars are hard to identify with IR and optical techniques. Recently, surveys of X-ray emission, especially with the German ROSAT satellite, have enabled detection of many stars that appear to be old or ...
... It has not been easy to find old T Tauri stars, in the 10- to 20-million-year range, because such stars are hard to identify with IR and optical techniques. Recently, surveys of X-ray emission, especially with the German ROSAT satellite, have enabled detection of many stars that appear to be old or ...
Processing of Star Catalog and Star Image
... areas in order to guarantee that the distribution of guide stars in the entire celestial area is as even as possible. Based on the single magnitude threshold, there are too many stars in the FOV as a result of some boresight pointings, while there are no stars in the FOV of some celestial areas. Obv ...
... areas in order to guarantee that the distribution of guide stars in the entire celestial area is as even as possible. Based on the single magnitude threshold, there are too many stars in the FOV as a result of some boresight pointings, while there are no stars in the FOV of some celestial areas. Obv ...
Chapter 17--Star Stuff
... The length of time from the formation of a protostar to the birth of a main-sequence star depends on the star’s mass. Massive stars do everything faster. The contraction of a high-mass protostar into a main-sequence star may take only a million years or less. A star like our Sun takes about 50 milli ...
... The length of time from the formation of a protostar to the birth of a main-sequence star depends on the star’s mass. Massive stars do everything faster. The contraction of a high-mass protostar into a main-sequence star may take only a million years or less. A star like our Sun takes about 50 milli ...
Asteroid Rotation Periods
... of a magnitude have been used. Even higher precision can be used, but this is not justified for measurements made by the eye alone, since the accuracy is about ½mag, and this is why the magnitude scale at first had only integer values. However today with the use of electronic sensors it is possible ...
... of a magnitude have been used. Even higher precision can be used, but this is not justified for measurements made by the eye alone, since the accuracy is about ½mag, and this is why the magnitude scale at first had only integer values. However today with the use of electronic sensors it is possible ...
Galaxies
... a. contain a large number of very young stars, but very little evidence of gas clouds. b. contain a large number of very old stars and almost no gas or dust. c. are often associated with a galaxy that is colliding with another galaxy. d. are common in rich clusters. e. are composed of filaments and ...
... a. contain a large number of very young stars, but very little evidence of gas clouds. b. contain a large number of very old stars and almost no gas or dust. c. are often associated with a galaxy that is colliding with another galaxy. d. are common in rich clusters. e. are composed of filaments and ...
CHAPTER 1 The Formation and Structure of Stars
... – Temperature is a measure of the motion of the atoms or molecules in a material—in a hot gas, the atoms move more rapidly than do those in a cool gas. – Although the interstellar clouds are very cold, even at a temperature of only 10 K, the average hydrogen atom moves about 0.5 km/s (1,100 mph). – ...
... – Temperature is a measure of the motion of the atoms or molecules in a material—in a hot gas, the atoms move more rapidly than do those in a cool gas. – Although the interstellar clouds are very cold, even at a temperature of only 10 K, the average hydrogen atom moves about 0.5 km/s (1,100 mph). – ...
The first carbon-enhanced metal-poor star found in the Sculptor
... first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way. Here we present detailed abundances from ESO VLT/UVES high-resolution spectroscopy for ET0097, the first CEMP star found in t ...
... first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way. Here we present detailed abundances from ESO VLT/UVES high-resolution spectroscopy for ET0097, the first CEMP star found in t ...
Stars: Intro & Classification Astronomy 1 — Elementary Astronomy LA Mission College
... We intentionally do not suggest that there is a simple mechanism for accomplishing this and we avoid the concept of filters. ...
... We intentionally do not suggest that there is a simple mechanism for accomplishing this and we avoid the concept of filters. ...
Ptolemy: on trial for fraud
... ogue, the Almagest. the ancient world, had committed a crime emy’s catalogue, howthe 16th century, by Lalande in the 18th cenagainst his fellow scientists and scholars, ever, contains 1022 stars. Dreyer and others tury, and also by Delambre. Was Ptolemy the betraying the ethics and integrity of his ...
... ogue, the Almagest. the ancient world, had committed a crime emy’s catalogue, howthe 16th century, by Lalande in the 18th cenagainst his fellow scientists and scholars, ever, contains 1022 stars. Dreyer and others tury, and also by Delambre. Was Ptolemy the betraying the ethics and integrity of his ...
Evolution of stars
... e. they are all so far away that the light hasn't reached us yet. The nuclear reactions in a star's core remain under control so long as a. luminosity depends on mass. b. pressure depends on temperature. c. density depends on mass. d. weight depends on temperature. e. temperature depends on mass. In ...
... e. they are all so far away that the light hasn't reached us yet. The nuclear reactions in a star's core remain under control so long as a. luminosity depends on mass. b. pressure depends on temperature. c. density depends on mass. d. weight depends on temperature. e. temperature depends on mass. In ...
Fluorine abundances in dwarf stars of the solar neighbourhood⋆
... Cloud and in the globular cluster ω Cen. They found that the abundance ratio of F/O declines as the oxygen abundance decreases. They therefore suggested that the observed low values of F/O exclude AGB synthesis as the dominant source of fluorine in their targeted stellar populations. In particular, ...
... Cloud and in the globular cluster ω Cen. They found that the abundance ratio of F/O declines as the oxygen abundance decreases. They therefore suggested that the observed low values of F/O exclude AGB synthesis as the dominant source of fluorine in their targeted stellar populations. In particular, ...
Life Histories Of Some Stars
... all? Describe the shape of the graph? Is it a straight line? A curve? 5. Give each group the list of stars attached and the HR diagram attached. Instead of height and weight, the information is in Luminosity (compared to sun) and Surface Temperature (in K). The chart also gives the star’s current st ...
... all? Describe the shape of the graph? Is it a straight line? A curve? 5. Give each group the list of stars attached and the HR diagram attached. Instead of height and weight, the information is in Luminosity (compared to sun) and Surface Temperature (in K). The chart also gives the star’s current st ...
Properties of Wolf-Rayet Stars - Paul Crowther, University of Sheffield
... WR stars can readily be obtained (e.g. Willis et al. 2004). Alternatively, optical and near-IR He i P Cygni profiles or mid-IR fine-structure metal lines may be used to derive reliable wind velocities (Howarth & Schmutz 1992; Dessart et al. 2000), for which the radial dependence is assumed to follow ...
... WR stars can readily be obtained (e.g. Willis et al. 2004). Alternatively, optical and near-IR He i P Cygni profiles or mid-IR fine-structure metal lines may be used to derive reliable wind velocities (Howarth & Schmutz 1992; Dessart et al. 2000), for which the radial dependence is assumed to follow ...
Starburst Galaxies - Beck-Shop
... the sky – rivalling galaxies – and the well-known Orion Nebula (M 42, Fig. 2.1) is exactly just such a region that has developed on the nearest side to us of the Orion GMC. The young stars, that can now be seen directly, have masses ranging from 0.08 solar masses (the brown dwarf limit) to slightly ...
... the sky – rivalling galaxies – and the well-known Orion Nebula (M 42, Fig. 2.1) is exactly just such a region that has developed on the nearest side to us of the Orion GMC. The young stars, that can now be seen directly, have masses ranging from 0.08 solar masses (the brown dwarf limit) to slightly ...
Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of
... Beirut. Finally I would like to thank all people and especially my family for their help, support and patience during the time I spent working on this project. ...
... Beirut. Finally I would like to thank all people and especially my family for their help, support and patience during the time I spent working on this project. ...
Astronomy Astrophysics
... orbit around the white dwarf. This scenario could also be valid for WD 0518+333 and might explain why different methods of analysis give such disparate results. The low gravity derived by Bergeron et al. (2001) is not covered by our model grid. Therefore some extrapolation was inevitable. Despite the ...
... orbit around the white dwarf. This scenario could also be valid for WD 0518+333 and might explain why different methods of analysis give such disparate results. The low gravity derived by Bergeron et al. (2001) is not covered by our model grid. Therefore some extrapolation was inevitable. Despite the ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.